Constraints on the Formation of M31's Stellar Halo from the SPLASH Survey

galaxies Conference Report Constraints on the Formation of M31’s Stellar Halo from the SPLASH Survey Karoline Gilbert 1,2 ID 1 Space Telescope Science Institute, 3700 San Martin Dr, Baltimore, MD 21218, USA; [email protected]; Tel.: +1-410-338-2475 2 Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA Academic Editors: Duncan A. Forbes and Ericson D. Lopez Received: 16 August 2017; Accepted: 13 September 2017; Published: 30 September 2017 Abstract: The SPLASH (Spectroscopic and Photometric Landscape of Andromeda’s Stellar Halo) Survey has observed fields throughout M31’s stellar halo, dwarf satellites, and stellar disk. The observations and derived measurements have either been compared to predictions from simulations of stellar halo formation or modeled directly in order to derive inferences about the formation and evolution of M31’s stellar halo. We summarize some of the major results from the SPLASH survey and the resulting implications for our understanding of the build-up of M31’s stellar halo. Keywords: galaxies: evolution; galaxies: halos; galaxies: individual (M31) 1. Introduction Observations of stellar halos provide the potential to decipher both the early and recent merger histories of nearby galaxies (Figure1). Recent accretion events are visible as strong enhancements in stellar density, and typically as kinematically cold features in stellar velocity distributions. These features can be modeled in detail to determine the properties of the progenitor system and its orbit (e.g., [1]). Simulations of stellar halo formation in a cosmological context make predictions for the global properties (e.g., stellar density profiles, metallicity gradients, and fraction of stars formed in situ and accreted) of stellar halos for hosts spanning a range of masses and merger histories (e.g., [2–5]). Suites of simulated stellar halos enable comparisons of the observed global properties of stellar halos to simulations to make inferences about the early accretion history of the halos. The proximity of the Andromeda galaxy (M31) provides a unique opportunity to study the global properties of a stellar halo in great detail. The ability to make measurements of individually resolved stars is powerful, enabling measurements of the stellar density to very low surface brightness, stellar line of sight velocities, chemical abundances, and star formation histories. This has led to a significant investment of time spent observing M31, including by the SPLASH (Spectroscopic and Photometric Landscape of Andromeda’s Stellar Halo), PAndAS (Pan-Andromeda Archaeological Survey; e.g., [6,7]), and PHAT (Panchromatic Hubble Andromeda Treasury; [8]) teams. Here we summarize the contributions to understanding the formation and evolution of M31’s stellar halo made by the SPLASH survey. Galaxies 2017, 5, 59; doi:10.3390/galaxies5040059 www.mdpi.com/journal/galaxies Galaxies 2017, 5, 59 2 of 10 Figure 1. A summary of what can be learned from observations of stellar halos. The underlying figure (Figure 2 of [9]) portrays the stellar surface density of M31’s stellar halo, and was generated from resolved star counts derived from images obtained with the MegaCam instrument on the Canada-France-Hawaii Telescope by the PAndAS survey [6]. 2. The SPLASH Survey The SPLASH collaboration has obtained photometry and spectroscopy of fields throughout M31’s stellar halo and disk. Photometry was primarily obtained with the Mosaic camera on the Kitt Peak 4 m Mayall Telescope, imaging 78 fields in the broad-band M and T2 filters, and the narrow-band DDO51 filter (PIs S. Majewski and R. Beaton). The DDO51 filter overlaps the surface-gravity-sensitive Mg b and MgH stellar ab-sorption features, which are strong in dwarf stars but weak in red giant branch (RGB) stars. This filter combination allows for the photometric pre-selection of stars likely to be M31 red giant branch stars (e.g., [10]), greatly increasing our spectroscopic efficiency over a large region of M31’s stellar halo. We have also utilized broad-band photometry obtained with SuprimeCam on Subaru, and Hubble Space Telescope imaging of M31’s disk. Spectroscopy of individual stars was obtained with the DEIMOS spectrograph on the Keck II 10 m telescope, primarily at R ∼ 6000. The SPLASH collaboration has obtained more than 20,000 M31 stellar spectra in ∼170 spectroscopic masks targeting Andromeda’s disk, dwarf galaxies, and halo, in fields ranging from 2 to 230 kpc in projected distance from Andromeda’s center (Figure2). The SPLASH dataset has led to the discovery and characterization of Andromeda’s extended metal-poor stellar halo [11–14]. In addition to the studies discussed below (global properties, identification and characterization of tidal debris features), it has also been used to study Andromeda’s dwarf satellites [15–21] and to characterize M31’s stellar disk [22]. Galaxies 2017, 5, 59 3 of 10 Figure 2. The locations of M31 halo and disk spectroscopic fields in the SPLASH survey. (Left) Fields targeting M31’s halo, tidal debris features, and dwarf galaxies, superimposed on a stellar density map created from the Pan-Andromeda Archaeological Survey (PAndAS) observations [23] (Figure 2 of Gilbert et al. [9]). (Right) Fields targeting M31’s disk; many of these spectroscopic masks were designed using photometry from the Hubble Space Telescope Multi Cycle Treasury Program PHAT (Figure 3 of Dorman et al. [24]). 3. The Properties of M31’s Halo Measured by SPLASH Below, we briefly summarize a selection of measurements made with the SPLASH dataset and their implications for the formation and evolution of Andromeda and its stellar halo. In each study, spectroscopic and photometric measurements were used to identify secure samples of M31 RGB stars, enabling us to remove Milky Way dwarf star contaminants (e.g., [12]). The stellar velocity distributions in each field were used to identify stars that were likely to be associated with kinematically cold tidal debris features (e.g., [25–27]). 3.1. Global Properties of Andromeda’s Stellar Halo 3.1.1. Surface Brightness and Metallicity Profiles SPLASH observations in 38 halo fields, spanning all quadrants of the halo and ranging from 9 to 230 kpc in projected distance from the center of M31 (Figure2), have been used to measure the surface brightness and metallicity profiles of M31’s stellar halo. The surface brightness profile of Andromeda’s stellar halo is consistent with a single power-law with a power law index of −2.2 ± 0.2, extending to a projected distance of more than 175 kpc from M31’s center (Figure3;[ 27]). This is true regardless of whether tidal debris features are included in the profile, although the inclusion of tidal debris features does affect the normalization and index of the power-law fit. A similar surface brightness profile was found using the PAndAS star count data [7], and an extension of a power-law profile into the inner regions of M31 (to 3 kpc in projected distance from M31’s center) was observed in blue horizontal branch stars with PHAT data [28,29]. There is no sign of a downward break in the surface brightness profile, out to ∼2/3 of the estimated virial radius (∼260 kpc; [30]). This was found to be atypical of simulated stellar halos, most of which do display a break in the surface brightness profile well within the range of projected radii probed by the SPLASH dataset. In the Bullock and Johnston [2] simulated halos, the only halo without a downward break in the stellar density profile is the one with many recent low-mass accretions. Future observations of the outer halo of M31—including measurements of the [Fe/H] and [a/Fe] abundances [31,32]—could confirm whether the stars in the outer halo are consistent with such a scenario: the mean [Fe/H] of a dwarf galaxy is strongly correlated with its luminosity (e.g., [33]), Galaxies 2017, 5, 59 4 of 10 while the [a/Fe] abundance is sensitive to the timescale over which stars formed (e.g., [34]). Together, the [Fe/H] and [a/Fe] abundances of halo stars can thus be used to infer the luminosity and time since accretion of the dwarf satellite progenitors (e.g., [1,2,35]). The SPLASH data also reveal that Andromeda’s stellar halo has a significant gradient in metallicity out to projected distances of ∼100 kpc [36], with a total decrease of ∼1 dex. A significant gradient is observed whether or not tidal debris features are included in the measurement. The [Fe/H] measurements shown in Figure3 are for a spectroscopically selected set of M31 RGB stars, but are based on photometry. Spectroscopic estimates of [Fe/H] for a subset of the highest S/N spectra, based on the equivalent width of the calcium triplet, result in a consistent gradient of metallicity with radius. A decrease in metallicity with radius was also observed in the PAndAS data [7]. Figure 3. (a) The surface brightness profile of M31’s stellar halo from the SPLASH survey (Figure 6 of Gilbert et al. [27]). The number of spectroscopically confirmed M31 RGB and Milky Way (MW) dwarf stars is used to determine the surface brightness in each SPLASH spectroscopic field. The surface brightness profile of halo stars after tidal debris features have been removed follows an r−2.2 power law to large distances from M31’s center. (b) Metallicity profile of M31’s stellar halo from the SPLASH survey (Figure 10 of Gilbert et al. [36]). Metallicity estimates are based on comparing the position of the star in the color magnitude diagram to a grid of isochrones at the distance of M31. All spectroscopically confirmed M31 RGB stars that are not associated with tidal debris features are shown as small, open black points; the median metallicity and estimated uncertainty in the median value are shown as large, solid red circles (fields without tidal debris features) and blue squares (fields with tidal debris features).

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